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Table 2

Parameters of the late WN stars from M 31

M31WRa LGGS Subtype T ∗ log Rt ν∞ E B − V M V R ∗ log Ṁ log L M ν b η c d M hom e M He - b f X H Comments
[kK] [R⊙] [kK] [km s-1] [mag] [mag] [R⊙] [M⊙/yr] [L⊙] [mag] [km s-1] [M⊙] [M⊙] [%]
17 J004024.33+405016.2 WN9 34 1.20 32 500 0.12 −5.62 14.1 −5.08 5.40 −5.80 0.82 −200 27 14 35
25 J004036.76+410104.3 WN8 50 0.80 37 500 0.15 −5.12 7.7 −4.87 5.52 −5.40 0.99 −100 32 16 35
27 J004056.49+410308.7 WN9 33 1.20 30 300 0.20 −6.93 26.5 −4.89 5.90 −7.15 0.24 −200 60 27 50
38 J004126.11+411220.0 WN7 40 0.95 33 1000 0.45 −6.87 19.9 −4.18 5.95 −6.92 3.68 −150 45 30 20
39 J004126.39+411203.5 WN8 40 0.95 31 300 0.55 −5.98 12.6 −5.00 5.55 −5.99 0.42 −100 39 17 50
42 J004130.37+410500.9 WN7−8g 35 1.40 35 300 0.22 −6.58 23.7 −5.26 5.90 −6.88 0.10 −175 42 27 20 +nebula
57 J004238.90+410002.0 WN7 40 1.00 34 1000 0.85 −6.28 14.9 −4.44 5.70 −6.24 3.58 −100 32 21 20
60 J004242.33+413922.7 WN10 25 0.80 17 300 0.30 −6.77 25.1 −4.32 5.35 −6.86 3.13 0 21 13 20
67 J004302.05+413746.7 WN9 35 1.10 31 500 0.75 −6.58 21.1 −4.66 5.80 −6.78 0.84 0 44 24 35
83 J004337.10+414237.1 WN10 25 1.00 19 500 0.30 −5.90 18.8 −4.59 5.10 −6.09 5.03 0 20 9 35
85 J004344.48+411142.0 WN8 35 1.20 33 400 0.40 −6.01 15.8 −5.10 5.55 −6.10 0.44 0 39 17 50 +nebula
88 J004353.34+414638.9 WN7 50 0.80 38 1000 0.10 −5.74 9.4 −4.44 5.70 −5.81 3.58 0 32 21 20
89 J004357.31+414846.2 WN8 45 0.70 30 500 0.70 −6.03 10.6 −4.51 5.60 −6.09 1.89 0 28 18 20
97 J004413.06+411920.5 WN8 35 1.40 35 500 0.35 −6.58 23.7 −5.04 5.90 −6.89 0.28 0 50 27 35
109 J004430.04+415237.1 WN8 35 1.50 35 1000 0.45 −6.53 21.1 −4.96 5.80 −6.64 0.85 200 53 24 50 diluted?
131 J004511.21+420521.7 WN11 22 1.20 20 300 0.30 −6.69 31.5 −4.77 5.35 −6.87 1.11 100 26 13 35
148 J004542.26+414510.1 WN10 28 1.00 22 500 0.75 −7.38 33.4 −4.21 5.80 −7.52 2.38 100 44 24 35

Notes.

(a)

The M31WR numbers correspond to the sequence of entries in Table 5 from Neugent et al. (2012) which is sorted by right ascension.

(b)

Absolute monochromatic magnitude Mν as defined by Smith (1968), reconstructed with our model SED.

(c)

The wind efficiency parameter η is defined as the ratio of wind and photon momentum: .

(d)

Peculiar radial velocity, , describing the radial velocity of the star in addition to the mean radial velocity of M 31 (−301  km s-1).

(e)

Current masses calculated from luminosity via the relation from Gräfener et al. (2011), which takes the different hydrogen fractions into account. These masses are based on the assumptions of a chemically homogeneous star.

(f)

Current mass calculated from luminosity via Gräfener et al. (2011) for a helium-burning star with a negligible mass of the hydrogen-containing outer layers.

(g)

Own classification.

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